On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances
- Autores
- Henry, R. B. C.; Stephenson, B. G.; Miller Bertolami, Marcelo Miguel; Kwitter, K. B.; Balick, B.
- Año de publicación
- 2018
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The primary goal of this paper is to make a direct comparison between the measured and model-predicted abundances of He, C, and N in a sample of 35 well-observed Galactic planetary nebulae (PNe). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4M⊙) were inferred using two published sets of post-asymptotic giant branch model tracks and L and Teff values. We conclude the following: (1) the mean values of N/O across the progenitor mass range exceeds the solar value, indicating significant N enrichment in the majority of our objects; (2) the onset of hot bottom burning appears to begin around 2 M⊙, i.e. lower than ~5M⊙ implied by theory; (3) most of our objects show a clear He enrichment, as expected from dredge-up episodes; (4) the average sample C/O value is 1.23, consistent with the effects of third dredge up; and (5) model grids used to compare to observations successfully span the distribution over metallicity space of all C/O and many He/H data points but mostly fail to do so in the case of N/O. The evident enrichment of N in PN and the general discrepancy between the observed and model-predicted N/O abundance ratios signal the need for extra mixing as an effect of rotation and/or thermohaline mixing in the models. The unexpectedly high N enrichment that is implied here for low-mass stars, if confirmed, will likely impact our conclusions about the source of N in the Universe.
Fil: Henry, R. B. C.. Oklahoma State University; Estados Unidos
Fil: Stephenson, B. G.. Oklahoma State University; Estados Unidos
Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Kwitter, K. B.. Williams College; Estados Unidos
Fil: Balick, B.. University of Washington; Estados Unidos - Materia
-
GALAXIES: ABUNDANCES
GALAXIES: ISM
ISM: ABUNDANCES
PLANETARY NEBULAE: GENERAL
STARS: AGB AND POST-AGB
STARS: EVOLUTION - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/82516
Ver los metadatos del registro completo
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On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundancesHenry, R. B. C.Stephenson, B. G.Miller Bertolami, Marcelo MiguelKwitter, K. B.Balick, B.GALAXIES: ABUNDANCESGALAXIES: ISMISM: ABUNDANCESPLANETARY NEBULAE: GENERALSTARS: AGB AND POST-AGBSTARS: EVOLUTIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The primary goal of this paper is to make a direct comparison between the measured and model-predicted abundances of He, C, and N in a sample of 35 well-observed Galactic planetary nebulae (PNe). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4M⊙) were inferred using two published sets of post-asymptotic giant branch model tracks and L and Teff values. We conclude the following: (1) the mean values of N/O across the progenitor mass range exceeds the solar value, indicating significant N enrichment in the majority of our objects; (2) the onset of hot bottom burning appears to begin around 2 M⊙, i.e. lower than ~5M⊙ implied by theory; (3) most of our objects show a clear He enrichment, as expected from dredge-up episodes; (4) the average sample C/O value is 1.23, consistent with the effects of third dredge up; and (5) model grids used to compare to observations successfully span the distribution over metallicity space of all C/O and many He/H data points but mostly fail to do so in the case of N/O. The evident enrichment of N in PN and the general discrepancy between the observed and model-predicted N/O abundance ratios signal the need for extra mixing as an effect of rotation and/or thermohaline mixing in the models. The unexpectedly high N enrichment that is implied here for low-mass stars, if confirmed, will likely impact our conclusions about the source of N in the Universe.Fil: Henry, R. B. C.. Oklahoma State University; Estados UnidosFil: Stephenson, B. G.. Oklahoma State University; Estados UnidosFil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Kwitter, K. B.. Williams College; Estados UnidosFil: Balick, B.. University of Washington; Estados UnidosOxford University Press2018-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82516Henry, R. B. C.; Stephenson, B. G.; Miller Bertolami, Marcelo Miguel; Kwitter, K. B.; Balick, B.; On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 473; 1; 1-2018; 241-2600035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stx2286info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/473/1/241/4107117info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:52:50Zoai:ri.conicet.gov.ar:11336/82516instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:52:51.263CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| title |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| spellingShingle |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances Henry, R. B. C. GALAXIES: ABUNDANCES GALAXIES: ISM ISM: ABUNDANCES PLANETARY NEBULAE: GENERAL STARS: AGB AND POST-AGB STARS: EVOLUTION |
| title_short |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| title_full |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| title_fullStr |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| title_full_unstemmed |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| title_sort |
On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances |
| dc.creator.none.fl_str_mv |
Henry, R. B. C. Stephenson, B. G. Miller Bertolami, Marcelo Miguel Kwitter, K. B. Balick, B. |
| author |
Henry, R. B. C. |
| author_facet |
Henry, R. B. C. Stephenson, B. G. Miller Bertolami, Marcelo Miguel Kwitter, K. B. Balick, B. |
| author_role |
author |
| author2 |
Stephenson, B. G. Miller Bertolami, Marcelo Miguel Kwitter, K. B. Balick, B. |
| author2_role |
author author author author |
| dc.subject.none.fl_str_mv |
GALAXIES: ABUNDANCES GALAXIES: ISM ISM: ABUNDANCES PLANETARY NEBULAE: GENERAL STARS: AGB AND POST-AGB STARS: EVOLUTION |
| topic |
GALAXIES: ABUNDANCES GALAXIES: ISM ISM: ABUNDANCES PLANETARY NEBULAE: GENERAL STARS: AGB AND POST-AGB STARS: EVOLUTION |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The primary goal of this paper is to make a direct comparison between the measured and model-predicted abundances of He, C, and N in a sample of 35 well-observed Galactic planetary nebulae (PNe). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4M⊙) were inferred using two published sets of post-asymptotic giant branch model tracks and L and Teff values. We conclude the following: (1) the mean values of N/O across the progenitor mass range exceeds the solar value, indicating significant N enrichment in the majority of our objects; (2) the onset of hot bottom burning appears to begin around 2 M⊙, i.e. lower than ~5M⊙ implied by theory; (3) most of our objects show a clear He enrichment, as expected from dredge-up episodes; (4) the average sample C/O value is 1.23, consistent with the effects of third dredge up; and (5) model grids used to compare to observations successfully span the distribution over metallicity space of all C/O and many He/H data points but mostly fail to do so in the case of N/O. The evident enrichment of N in PN and the general discrepancy between the observed and model-predicted N/O abundance ratios signal the need for extra mixing as an effect of rotation and/or thermohaline mixing in the models. The unexpectedly high N enrichment that is implied here for low-mass stars, if confirmed, will likely impact our conclusions about the source of N in the Universe. Fil: Henry, R. B. C.. Oklahoma State University; Estados Unidos Fil: Stephenson, B. G.. Oklahoma State University; Estados Unidos Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Kwitter, K. B.. Williams College; Estados Unidos Fil: Balick, B.. University of Washington; Estados Unidos |
| description |
The primary goal of this paper is to make a direct comparison between the measured and model-predicted abundances of He, C, and N in a sample of 35 well-observed Galactic planetary nebulae (PNe). All observations, data reductions, and abundance determinations were performed in house to ensure maximum homogeneity. Progenitor star masses (M ≤ 4M⊙) were inferred using two published sets of post-asymptotic giant branch model tracks and L and Teff values. We conclude the following: (1) the mean values of N/O across the progenitor mass range exceeds the solar value, indicating significant N enrichment in the majority of our objects; (2) the onset of hot bottom burning appears to begin around 2 M⊙, i.e. lower than ~5M⊙ implied by theory; (3) most of our objects show a clear He enrichment, as expected from dredge-up episodes; (4) the average sample C/O value is 1.23, consistent with the effects of third dredge up; and (5) model grids used to compare to observations successfully span the distribution over metallicity space of all C/O and many He/H data points but mostly fail to do so in the case of N/O. The evident enrichment of N in PN and the general discrepancy between the observed and model-predicted N/O abundance ratios signal the need for extra mixing as an effect of rotation and/or thermohaline mixing in the models. The unexpectedly high N enrichment that is implied here for low-mass stars, if confirmed, will likely impact our conclusions about the source of N in the Universe. |
| publishDate |
2018 |
| dc.date.none.fl_str_mv |
2018-01 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
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publishedVersion |
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http://hdl.handle.net/11336/82516 Henry, R. B. C.; Stephenson, B. G.; Miller Bertolami, Marcelo Miguel; Kwitter, K. B.; Balick, B.; On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 473; 1; 1-2018; 241-260 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/82516 |
| identifier_str_mv |
Henry, R. B. C.; Stephenson, B. G.; Miller Bertolami, Marcelo Miguel; Kwitter, K. B.; Balick, B.; On the production of He, C, and N by low- and intermediate-mass stars: A comparison of observed and model-predicted planetary nebula abundances; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 473; 1; 1-2018; 241-260 0035-8711 CONICET Digital CONICET |
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eng |
| language |
eng |
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openAccess |
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